J/A+A/680/A32ivo://CDS.VizieR/J/A+A/680/A32doi:10.26093/cds/vizier.36800032CDSBodensteiner J.Sana H.Dufton P.L.Wang C.Langer N.Banyard G.,Mahy L.de Koter A.de Mink S.E.Evans C.J.Goetberg Y.,Henault-Brunet V.Patrick L.R.Schneider F.R.N.2025-05-06T20:01:04Z2023-12-07T09:01:52ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frmagellanic-cloudsopen-star-clustersvisible-astronomyinfrared-astronomyThe origin of initial rotation rates of stars, and how a star's surface rotational velocity changes during the evolution, either by internal angular momentum transport or due to interactions with a binary companion, remain open questions in stellar astrophysics. Here, we aim to derive the physical parameters and study the distribution of (projected) rotational velocities of B-type stars in the 35 Myr-old, massive cluster NGC 330 in the Small Magellanic Cloud. NGC 330 is in an age range where the number of post-interaction binaries is predicted to be high near the cluster turnoff (TO). We develop a simultaneous photometric and spectroscopic grid-fitting method adjusting atmosphere models on multi-band Hubble Space Telescope photometry and Multi Unit Spectroscopic Explorer spectroscopy. This allows us to homogeneously constrain the physical parameters of over 250 B and Be stars, brighter than mF814W=18.8mag. The rotational velocities of Be stars in NGC 330 are significantly higher than the ones of B stars. The rotational velocities vary as a function of the star's position in the color-magnitude diagram, qualitatively following predictions of binary population synthesis. A comparison to younger clusters shows that stars in NGC 330 rotate more rapidly on average. The rotational velocities of the 35Myr old population in NGC 330 quantitatively agree with predictions for a stellar population that underwent significant binary interactions: the bulk of the B stars could be single stars or primaries in pre-interaction binaries. The rapidly spinning Be stars could be mass and angular momentum gainers in previous interactions, while those Be stars close to the TO may be spun-up single stars. The slowly rotating, apparently single stars above the TO could be merger products. The different vsini-characteristics of NGC 330 compared to younger populations can be understood in this framework.2023A&A...680A..32Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/680/A32CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/634/A51 : NGC 330 seen by MUSE I. (Bodensteiner+, 2020)J/A+A/652/A70 : NGC 330 seen by MUSE II. (Bodensteiner+, 2021)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/680/A32https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/680/A32http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/680/A32https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/680/A32https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/680/A32http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/680/A32GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/680/A32/tablea1 (Compilation of all parameters derived for the stars)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/680/A32/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/680/A32/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/680/A32/tablea1?GETtext/xml+votable180.050000true14.07891306-72.472821940.0055555555555555566/333172.0401237512456292e-19 7.605786964834612e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/680/A32?format=asciiOpticalInfrareddefaultJ/A+A/680/A32/tablea1Compilation of all parameters derived for the starsE_Rad? Radius, upper errorsolRadstat.error;stat.maxfloatnullableSimbadSimbad column added by the CDSmeta.ref.urlcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintID[10/732] Identification numbermeta.id;meta.mainintRAJ2000Right ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Declination (J2000)degpos.eq.dec;meta.mainF336WF336W magnitude from (Milone et al., 2018MNRAS.477.2640M)magphot.mag;em.opt.UfloatF814WF814W magnitude from (Milone et al., 2018MNRAS.477.2640M)magphot.mag;em.opt.IfloatSpTypeSpectral typesrc.spTypecharTeffEffective temperature TeffKphys.temperature.effectiveintE_Teff? Effective temperature, upper errorKstat.error;stat.maxintnullablee_Teff? Effective temperature, lower errorKstat.error;phys.temperature.effectiveintnullableloggSurface gravity logglog(cm.s**-2)phys.gravityfloatE_logg? Surface gravity, upper errorlog(cm.s**-2)stat.error;stat.maxfloatnullablee_logg? Surface gravity, lower errorlog(cm.s**-2)stat.errorfloatnullablevsiniProjected rotational velocity vsinikm/sphys.veloc.rotatintE_vsini? Projected rotational velocity, upper errorkm/sstat.error;stat.maxintnullablee_vsini? Projected rotational velocity, lower errorkm/sstat.error;phys.veloc.rotatintnullableRadRadiussolRadphys.size.radiusfloate_Rad? Radius, lower errorsolRadstat.errorfloatnullableLumLuminositysolLumphys.luminosityfloatE_Lum? Luminosity, upper errorsolLumstat.error;stat.maxfloatnullablee_Lum? Luminosity, lower errorsolLumstat.errorfloatnullableFlagBinary flag (1)meta.code.errorchar